%% Issue 119, February 2007, of the Active Galaxies Newsletter is
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%% at:
%%
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%% *********** NOTE THE NEW WEB & EMAIL ADDRESS ABOVE ****************
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%% This new issue is also included below in its LaTeX version.
%%
%%
%% ********** IMPORTANT CHANGES TO THE NEWSLETTER ***********
%%
%%
%% Please note that the web & email addresses for the Active
%% Galaxies Newsletter has changed. This is part of a
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%% This will be announced in due course. In the immediate future
%% the old web & email address will for forward to the new
%% addresses but please make note of the new address and change
%% your bookmarks.
%%
%% ************ A NEW SECTION FOR THE NEWSLETTER ***********
%%
%% ********* Submitted papers for discussion ***********
%%
%% It has recently been suggested to me by one of the contributers
%% and subscribers to the newsletter that a the inclusion of
%% recently submitted, but not refereed papers, in the newsletter
%% would be a useful addition. This section would allow authors to
%% disseminate there new and exciting work earlier to the community
%% and allow open discussion and feedback to the authors at an
%% early stage. As such from the next issue the newsletter will be
%% publishing abstracts, with associated web-links where the full
%% paper can be downloaded, of submitted but not accepted papers.
%% This will be an additional and separate section in the
%% newsletter and clearly labelled. In addition to the abstract
%% authors will be able to optionally include a short paragraph
%% with additional comments regarding the work. In addition to
%% appearing in the newsletter these contributions will also be
%% posted on the Newsletter's web-pages promptly following their
%% receipt.
%%
%% It is hoped that this new section will be popular and useful to
%% the subscribers and readers by allowing very prompt
%% dissemination and hence discussion of new results amongst a
%% targeted group of researchers.
%%
%%
%% As always as editor of the newsletter I am very interested to hear
%% any suggestions or feedback regarding the newsletter. So do not hesitate
%% in emailing me your suggestions.
%%
%% Many thanks for your continued subscription.
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%% Rob Beswick
%%
%%=====================================================================
%% Active Galaxies Newsletter
%% Web - http://www.manchester.ac.uk/jodrellbank/~agnews
%% Email enquiries & Submissions - agnews@manchester.ac.uk
%%--------------------------------------------------------------------
%% Dr Rob Beswick |
%% University of Manchester, |
%% Jodrell Bank Observatory, |
%% Macclesfield, Cheshire, | Email : Robert.Beswick@manchester.ac.uk
%% SK11 9DL, United Kingdom | Web : http://www.jb.man.ac.uk/~rbeswick/
%%=====================================================================
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\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Active}
& \multicolumn{1}{|c|}{\large\em An electronic publication dedicated to}\\ [0.3cm]
\multicolumn{1}{|l|}{\hspace{0.5cm}\LARGE\bf\sf Galaxies} & \multicolumn{1}{|c|}{\large\em the observation and theory of}\\ [0.3cm]
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\multicolumn{1}{|c|}{\large\bf\sf No. 119 --- February 2007 } &
\multicolumn{1}{|c|}{\bf\sf Editor: Rob Beswick (agnews@manchester.ac.uk)} \\ [-0.1cm]
& \\ \hline
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\small
\begin{center}
{\Large\em Accepted Abstracts - Submitted Abstracts - Thesis Abstracts\\
Jobs Adverts - Meetings Adverts - Special Announcements}
\end{center}
\begin{center}
{\Large\sf From the Editor}
\end{center}
\vspace*{0.6cm}
The Active Galaxies Newsletter is produced monthly. The deadline for
contributions is the last friday of the month. The Latex macros for
submitting abstracts and dissertation abstracts are appended to each
issue of the newsletter and are also available on the web page.
\begin{center}
{\bf IMPORTANT CHANGES TO THE NEWSLETTER}
\end{center}
Please note that the web \& email addresses for the Active Galaxies
Newsletter has changed. This is part of a rationalisation of servers at the
newsletter's host institute. This will be announced in due course. In the
immediate future the old web \& email address will for forward to the new
addresses but please make note of the new address and change your
bookmarks.
\vspace*{0.5cm}
{\large
{\bf THE NEW EMAIL ADDRESS IS: \hspace*{3cm} agnews@manchester.ac.uk}
\vspace*{0.3cm}
{\bf THE WEB-PAGE ADDRESS IS: \hspace*{0.3cm}
http://www.manchester.ac.uk/jodrellbank/$\sim$agnews}}
\vspace*{0.5cm}
\begin{center}
{\bf A NEW SECTION FOR THE NEWSLETTER:}
{\large\em Submitted papers for discussion }
\end{center}
It has recently been suggested to me by one of the contributers and
subscribers to the newsletter that a the inclusion of recently submitted,
but not refereed papers, in the newsletter would be a useful addition. This
section would allow authors to disseminate there new and exciting work
earlier to the community and allow open discussion and feedback to the
authors at an early stage. As such from the next issue the newsletter will
be publishing abstracts, with associated web-links where the full paper can
be downloaded, of submitted but not accepted papers. This will be an
additional and separate section in the newsletter and clearly labelled. In
addition to the abstract authors will be able to optionally include a short
paragraph with additional comments regarding the work. In addition to
appearing in the newsletter these contributions will also be posted on the
Newsletter's web-pages promptly following their receipt.
It is hoped that this new section will be popular and useful to the
subscribers and readers by allowing very prompt dissemination and hence
discussion of new results amongst a targeted group of researchers. A LaTeX
macro template for these new contributions will be available shortly from
the webpages.
As always as editor of the newsletter I am very interested to hear any
suggestions or feedback regarding the newsletter. So do not hesitate in
emailing me your suggestions.
Many thanks for your continued subscription.
\begin{center}
Rob Beswick
\end{center}
%\vspace*{1cm}
\newpage
\begin{center}
{\Large\sf Abstracts of recently accepted papers}
\end{center}
\vspace*{0.6cm}
{\large\bf{ The broad band spectrum and variability of NGC 4151 observed
by BeppoSAX}}
{\bf{ A. De Rosa$^1$, L. Piro$^1$, G.C Perola$^2$, M. Capalbi$^3$,
M. Cappi$^4$, P. Grandi$^4$, L. Maraschi$^5$ and P.O. Petrucci$^6$ }}
$^1$ {Istituto di Astrofisica Spaziale e Fisica Cosmica, INAF,
sezione di Roma, Via Fosso del Cavaliere, 00133 Roma, Italy} \\
$^2$ {Dipartimento di Fisica, Universit\`a degli
Studi ``Roma Tre'', Via della Vasca Navale 84, I--00146 Roma,
Italy} \\
$^3$ {ASI Science Data Center, c/o ESA-ESRIN, Via Galileo Galilei, 00044
Frascati, Italy}\\
$^4$ {Istituto di Astrofisica Spaziale e Fisica Cosmica, INAF, sezione di
Bologna, Via Gobetti 101, I-40129, Italy}\\
$^5$ {Osservatorio Astronomico di Brera, INAF, Via Brera 28, Milan
I-20121, Italy}\\
$^6$ {Laboratoire d'Astrophysique de Grenoble, BP 43, 38041
Grenoble Cedex 9, France }
\def\sax{{\it BeppoSAX~}}
\def\41{NGC~4151}
{We present an analysis of all \sax observations of \41. This source was
observed 5 times from 1996 to 2001 with durations ranging from a day to
four days. The intrinsic continuum (described as a cut-off power law) is
absorbed at low energies by a complex system: a cold patchy absorber plus a
warm uniform screen photoionised by the central continuum. We find that
this ``dual absorber'' is the main driver of the observed variability, up
to a factor of eight, at 3 keV. In particular the covering fraction of the
cold absorber changes on time scales of the order of a day, supporting its
association with the broad-line region. The column density of the warm gas
varies on a longer time scale (months to year). Some of the small amplitude
spectral variability above 10 keV can be explained with an intrinsic
variation (with variation of the photon index $\Delta\Gamma \sim 0.2$). The
flux below 1 keV remains constant confirming an extended origin. Its
spectrum is reproduced by a combination of a thermal component (with
temperature $kT=0.15$ keV) and a power law with the same slope as the
intrinsic continuum, but with an intensity of a few percent. A Compton
reflection component is significantly detected in 1996 (averaged value of
$\Omega/2\pi \sim0.4$, with the solid angle $\Omega$ covered by the
reflecting medium), with intensity decreasing on a time scale of a year,
and it desappears in 2000 and 2001. The long time scale of variations
argues for an association with an optically thick torus at a distance of a
few light years. An iron line was detected in all spectra. Its energy is
consistent with fluorescence by cold iron. We find that the line is
variable. Its behaviour is reproduced by a variable component proportional
to the level of the reflection flux plus a constant component. The flux of
the latter is consistent with the extended line emission observed by {\it
Chandra}. We conclude that the first component likely arises from the torus
and the second is produced in the extended narrow-line region.}
{ Accepted by Astronomy \& Astrophysics }
{E-mail contact: alessandra.derosa@iasf-roma.inaf.it,\newline preprint
available at
astro-ph/0611470 }
\vspace*{0.6cm}
{\large\bf{3D Radiative Transfer Modeling of Clumpy Dust Tori Around AGN}}
{\bf{ S.~F. H\"onig, T. Beckert, K. Ohnaka \ and G. Weigelt}}
{Max-Planck-Institut f\"ur Radioastronomie, Auf dem H\"ugel 69, 53121 Bonn, Germany}
{We present 3-dimensional radiative transfer models for clumpy dust tori
around AGN (see H\"onig et al. 2006, A\&A, 452, 459). Our method combines
Monte Carlo simulations of individual dust clouds with the actual
3-dimensional distribution of clouds in the torus. The model has been
applied to NIR and MIR photometric and interferometric observations of
NGC~1068. For the first time, it is possible to simultaneously reproduce
both photometric and interferometric observations in the NIR and MIR. We
infer a luminosity $L=2\times10^{45}\,{\rm erg/s}$ and an inclination of
$i=70\deg$ for NGC~1068 from our model.}
{To appear in ``The Central Engine of Active Galactic Nuclei'', ed. L.~C.
Ho and J.-M. Wang (San Francisco: Astronomical Society of the Pacific
2007)}
{E-mail contact: shoenig@mpifr-bonn.mpg.de,\newline preprint available at
http://arxiv.org/abs/astro-ph/0611946}
%\vspace*{0.6cm}
\newpage
{\large\bf{Modeling optical and UV polarization of AGNs I. Imprints of
individual scattering regions}}
{\bf{ Ren\'e W. Goosmann$^{1,2}$ \ and C. Martin Gaskell$^3$ }}
$^1$ {Astronomical Institute of the Academy of Sciences, Bo{\v c}ni II 1401,
14131 Prague, Czech Republic} \\
$^2$ {Observatoire de Paris - Meudon, 5 place Jules Janssen,
92190 Meudon, France} \\
$^3$ {Department of Physics \& Astronomy, University of Nebraska,
Lincoln, NE 68588-0111, USA}
{Spectropolarimetry of AGNs is a powerful tool for studying the structure
and kinematics of the inner regions of quasars. We wish to investigate the
effects of various AGN scattering region geometries on the polarized flux.
We introduce a new, publicly available Monte Carlo radiative transfer code,
{\sc Stokes}, which models polarization induced by scattering off free
electrons and dust grains. We model a variety of regions in AGNs. We find
that the shape of the funnel of the dusty torus has a significant impact on
the polarization efficiency. A compact torus with a steep inner surface
scatters more light toward type-2 viewing angles than a large torus of the
same half-opening angle, $\theta_0$. For $\theta_0 < 53^\circ$, the
scattered light is polarized perpendicularly to the symmetry axis, whilst
for $\theta_0 > 60^\circ$ it is polarized parallel to the symmetry axis. In
between these intervals the orientation of the polarization depends on the
viewing angle. The degree of polarization ranges between 0\% and 20\% and
is wavelength-independent for a large range of $\theta_0$. Observed
wavelength-independent optical and near-UV polarization thus does not
necessarily imply electron scattering. Spectropolarimetry at rest-frame
wavelengths less than 2500~\AA~may distinguish between dust and electron
scattering but is not conclusive in all cases. For polar dust, scattering
spectra are reddened for type-1 viewing angles, and made bluer for type-2
viewing angles. Polar electron-scattering cones are very efficient
polarizers at type-2 viewing angles, whilst the polarized flux of the torus
is weak. We predict that the net polarization of Seyfert-2 galaxies
decreases with luminosity, and conclude that the degree of polarization
should be correlated with the relative strength of the thermal IR flux.
We find that a flattened, equatorial, electron-scattering disk, of
relatively low optical depth, reproduces type-1 polarization. This is
insensitive to the exact geometry, but the observed polarization requires a
limited range of optical depth.}
{ Accepted by Astronomy \& Astrophysics }
{E-mail contact: goosmann@astro.cas.cz,\newline preprint available at
astro-ph/0507072}
\vspace*{0.6cm}
{\large\bf{Reverberation Mapping of High-Luminosity Quasars: First Results}}
{\bf{ Shai~Kaspi$^{1,2}$, W. N. Brandt$^3$, Dan~Maoz$^1$, Hagai~Netzer$^1$,
Donald P. Schneider$^3$, and Ohad Shemmer$^3$ }}
$^1$ {School of Physics and Astronomy, Raymond and Beverly
Sackler Faculty of Exact Sciences, Tel-Aviv University, Tel-Aviv 69978,
Israel} \\
$^2$ {Physics Department, Technion, Haifa 32000, Israel} \\
$^3$ {Department of Astronomy and Astrophysics, 525 Davey
Laboratory, Pennsylvania State University, University Park, PA 16802}
\newcommand \gtorder {\mathrel{\raise.3ex\hbox{$>$}\mkern-14mu
\lower0.6ex\hbox{$\sim$}}}
{Reverberation mapping of nearby active galactic nuclei has led to
estimates of broad-line-region (BLR) sizes and central-object masses for
some 37 objects to date. However, successful reverberation mapping has yet
to be performed for quasars of either high luminosity (above $L_{\rm
opt}\sim 10^{46}~{\rm erg~s}^{-1}$) or high redshift ($z\gtorder$\,0.3).
Over the past six years, we have carried out, at the Hobby-Eberly
Telescope, rest-frame-ultraviolet spectrophotometric monitoring of a sample
of six quasars at redshifts $z=2.2-3.2$, with luminosities of $L_{\rm
opt}\sim 10^{46.4}$--$10^{47.6}~{\rm erg~s}^{-1}$, an order of magnitude
greater than those of previously mapped quasars. The six quasars, together
with an additional five having similar redshift and luminosity properties,
were monitored photometrically at the Wise Observatory during the past
decade. All 11 quasars monitored show significant continuum variations of
order 10--70\%. This is about a factor of two smaller variability than for
lower luminosity quasars monitored over the same rest-frame period. In the
six objects which have been spectrophotometrically monitored, significant
variability is detected in the C{\sc iv}$\lambda1550$ broad emission line.
In several cases the variations track the continuum variations in the same
quasar, with amplitudes comparable to, or even greater than, those of the
corresponding continua. In contrast, no significant Ly$\alpha$ variability
is detected in any of the four objects in which it was observed. Thus, UV
lines may have different variability trends in high-luminosity and
low-luminosity AGNs. For one quasar, S5\,0836+71 at $z=2.172$, we measure
a tentative delay of 595 days between C{\sc iv} and UV-continuum
variations, corresponding to a rest-frame \ delay of 188 days and a central
\ black-hole mass of $2.6\times10^9 M_{\odot}$. }
{ Accepted by ApJ }
{E-mail contact: shai@wise.tau.ac.il,\newline preprint available at
http://arXiv.org/abs/astro-ph/0612722}
%\vspace*{0.6cm}
\newpage
{\large\bf{Near-infrared spectra of Seyfert galaxies and line
production mechanisms 9 10}}
{\bf{N. Jackson and R. J. Beswick}}
{The University of Manchester, Jodrell Bank Observatory, Macclesfield,
Cheshire, SK11 9DL U.K.}
{New observations are reported of J-band spectra (1.04\,$\mu$m --
1.4\,$\mu$m) of three Seyfert 2 galaxies, Mkn 34, Mkn 78 and NGC 5929. In
each case the spectral range includes the near-infrared lines of [Fe{\sc
ii}], [P{\sc ii}], He{\sc i} and Pa$\beta$. Each Seyfert galaxy has a known
radio jet, and we investigate the infrared line ratios of the nuclear and
extended regions of each galaxy compared to the radio structure. In Mkn 34
there is a clear indication of an extranuclear region, probably coincident
with a shock induced by the radio jet, in which [Fe{\sc ii}] is
considerably enhanced, although the nuclear emission is almost certainly
the result of photoionization by the continuum of the active nucleus.
Similar effects in extranuclear regions are seen in the other objects, in
the case of Mkn 78 confirming recent studies by Ramos Almeida et al. A
possible detection of extranuclear [P{\sc ii}] emission suggests, if real,
that photoionization by the active nucleus is the dominant line excitation
mechanism over the whole source, including the regions coincident with the
radio jet.}
{ Accepted by MNRAS}
{E-mail contact: Robert.Beswick@manchester.ac.uk,\newline preprint
http://arXiv.org/abs/astro-ph/0701384}
\vspace*{0.6cm}
{\large\bf{An Update on the X-ray transient Narrow-Line Seyfert 1 galaxy
WPVS 007: {\it Swift} observations of UV variability and persistence
of X-ray faintness}}
{\bf{ Dirk Grupe$^{1}$,
Patricia Schady$^{1,2}$,
Karen M. Leighly$^{3}$,
Stefanie Komossa$^{4}$,
Paul T. O'Brien$^{5}$,
\& John A. Nousek$^{1}$}}
$^{1}$ {Department of Astronomy and Astrophysics, Pennsylvania State
University, 525 Davey Lab, University Park, PA 16802}\\
$^{2}$ {Mullard Space Science Laboratory, Holmbury St. Mary, Dorking,
Surrey RH5 6NT, U.K.; email: ps@mssl.ucl.ac.uk}\\
$^{3}$ {Homer L. Dodge Department of Physics and Astronomy, University of
Oklahoma, 440 West Brooks Street, Norman, OK 73019; email:
leighly@nhn.ou.edu}\\
$^{4}$ {MPI f\"ur extraterrestrische Physik, Giessenbachstr., D-85748
Garching,Germany; email: skomossa@mpe.mpg.de}\\
$^{5}$ {Department of Physics \& Astronomy, University of Leicester,
Leicester, LE1 7R, UK, email: pto@star.le.ac.uk}
{We report on the detection of UV variability and the persistence of X-ray
faintness of the X-ray transient Narrow-Line Seyfert 1 galaxy WPVS 007
based on the first year of monitoring this AGN with {\it Swift} between
2005 October and 2007 January. WPVS 007 has been an unusual source. While
being X-ray bright during the ROSAT All-Sky Survey it has been extremely
faint in all following X-ray observations. {\it Swift} also finds this NLS1
to be X-ray faint and not detected in the {\it Swift}~X-Ray Telescope at an
3$\sigma$ upper limit of $2.6\times 10^{-17}$ W m$^{-2}$ in the 0.3-10.0
keV band and confirms that the AGN is still in a low state. During the 2006
July and December observations with {\it Swift}'s UV-Optical Telescope
(UVOT) the AGN became fainter by about 0.2 mag in the UV filters and by
about 0.1 mag in V, B, and U compared with the 2005 October to 2006 January
and 2006 September/October observations followed by a rebrightening in the
2007 January observation. This variability can be caused either by a change
in the absorption column density and therefore the reddening in the UV, or
by flux variations of the central engine. We also noticed that the flux in
the UVOT filters agree with earlier measurements by the International
Ultraviolet Explorer taken between 1993-1995, but spectra taken by the
Hubble Space Telescope Faint Object Spectrograph show that WPVS 007 was
fainter in the UV by a factor of at least 2 in 1996. The flat optical/UV
spectrum suggests that some UV extinction is present in the spectrum, but
that alone cannot at all account for the dramatic fading in the X-ray flux.
Most likely we see a partial covering absorber in X-rays. Alternatively,
the current X-ray emission seen from WPVS 007 may also be the emission from
the host galaxy.}
{ Accepted for publication by the Astronomical Journal }
{E-mail contact: grupe@astro.psu.edu,\newline preprint available at
astro-ph/0701564}
\vspace*{0.6cm}
{\large\bf{FIRST `Winged' and `X'-shaped Radio Source Candidates}}
{\bf{ C.C. Cheung$^{1.,2}$}}
$^1$ {Jansky Postdoctoral Fellow, National Radio Astronomy Observatory}\\
$^2$ {Kavli Institute for Particle Astrophysics and Cosmology, Stanford
University, Stanford CA 94305}
{A small number of double-lobed radio galaxies (17 from our own census of
the literature) show an additional pair of low surface brightness `wings',
thus forming an overall `X'-shaped appearance. The origin of the wings in
these radio sources is unclear. They may be the result of back-flowing
plasma from the currently active radio lobes into an asymmetric medium
surrounding the active nucleus, which would make these ideal systems in
which to study thermal/non-thermal plasma interactions in extragalactic
radio sources. Another possibility is that the wings are the aging radio
lobes left over after a (rapid) realignment of the central supermassive
black-hole/accretion disk system due perhaps to a merger. Generally, these
models are not well tested; with the small number of known examples,
previous works focused on detailed case studies of selected sources with
little attempt at a systematic study of a large sample. Using the VLA-FIRST
survey database, we are compiling a large sample of winged and X-shaped
radio sources for such studies. As a first step toward this goal, an
initial sample of 100 new candidate objects of this type are presented in
this paper. The search process is described, optical identifications from
available literature data, and basic radio data are presented. From the
limited resolution FIRST images ($\sim$5''), we can already confidently
classify a sufficient number of these objects as having the characteristic
wing lengths $>$80$\%$ of the active lobes to more than double the number
of known X-shaped radio sources. We have also included as candidates,
radio sources with shorter wings ($ 1 \ \mu \rm m$) bandpasses. By comparing to
instantaneous burst, stellar population synthesis models (Bruzual \&
Charlot 2003), we estimate that most of the clusters are consistent with
being $\sim$15 Myr old and have photometric masses ranging from $7 \times
10^{5} \rm M_ {\odot}$ to $4 \times 10^{7} \rm M_{\odot}$. The total
contribution to the star formation rate (SFR) from these clusters is
approximately $10 \rm M_{\odot} \ yr^{-1}$, or $\sim$10\% of the total SFR
in the nuclear region. We use these newly discovered clusters to estimate
the extinction toward NGC 6240's double nuclei, and find values of $ \rm
A_{V}$ as high as 14 magnitudes along some sightlines, with an average
extinction of $\rm A_{V} \sim 7$ mag toward sightlines within $\sim3$
arcsec of the double nuclei.}
{Accepted by ApJ}
{E-mail contact: pollack@ucolick.org,\newline preprint available at
http://arxiv.org/abs/astro-ph/0701514}
\vspace*{0.6cm}
{\large\bf{The size of BLRs of low luminosity Active Galactic Nuclei}}
{\bf{ Xue-Guang Zhang$^{1,2}$, Dultzin-Hacyan D.$^1$ \ and Ting-Gui Wang$^2$ }}
$^1$ {Instituto de Astronom\'ia, Universidad Nacional Aut\'onoma de
M\'exico, Apdo Postal 70-264, M\'exico D. F. 04510, Mexico} \\
$^2$ {Center for Astrophysics, Department of astronomy and Applied
Physics, University of Science and Technology of China,
Hefei, Anhui, P.R.China}
{We study the size of BLRs of low luminosity Active Galactic Nuclei, also
called 'dwarf AGN', defined as having ($L_{H\alpha}\le10^{41}{\rm erg\cdot
s^{-1}}$). We more than double the sample size analyzed previously (Wang \&
Zhang 2003, hereafter Paper I). In this study we first confirm our previous
result that the sizes of BLRs of low luminosity AGN are larger than the
ones expected from the empirical relation $R_{BLRs} - L_{H\alpha}$ valid
for 'normal' AGN: Seyfert 1s and quasars, except for the objects with
accretion rate $\dot{m_{H\alpha}}>10^{-5.5}$. Second, we find a positive
correlation between the line width of the narrow emission line (as tracer
of velocity dipersion and thus bulge and black hole mass) and the size of
BLRs for both normal and low luminosity AGN. In this paper we find a
non-linear dependence of the BLRs sizes of low luminosity AGN on BH masses.
We also show that their sizes of BLRs are more strongly dominated by the
'specific accretion rate' $\dot{m_{H\alpha}}$ defined as $\dot{m_{H\alpha}}
= L_{H\alpha}/L_{Edd}$, than by the masses of their cetral black holes. {
As an expected result, the distance of emission regions of low-ionization
broad H$\alpha$ of NGC 4395 should be consistent with the value from the
empirical relation of $R_{BLRs} - L_{H\alpha}$, according to the high
accretion rate}
{ Accepted by MNRAS }
{E-mail contact: xguang@astroscu.unam.mx,\newline preprint available at
http://arxiv.org/abs/astro-ph/0610300}
\vspace*{0.6cm}
{\large\bf{The properties of optical FeII emission lines of AGN with
double-peaked broad emission lines}}
{\bf{ Xue-Guang Zhang$^{1,2}$, Dultzin-Hacyan D.$^1$ \ and Ting-Gui Wang$^2$ }}
$^1$ {Instituto de Astronom\'ia, Universidad Nacional Aut\'onoma de
M\'exico, Apdo Postal 70-264, M\'exico D. F. 04510, Mexico} \\
$^2$ {Center for Astrophysics, Department of astronomy and Applied
Physics, University of Science and Technology of China,
Hefei, Anhui, P.R.China}
{We study the FeII properties of double-peaked broad low-ionization
emission line AGN (dbp emitters) using a sample of 27 dbp emitters from
SDSS (DR4). Our first result is that the line spectra in the wavelength
range from 4100$\AA$ to 5800$\AA$ can be best fitted by an elliptical
accretion disk model. The best fitted results indicate that the optical
FeII emission lines of dbp emitters originate from the same region in the
accretion disk where the double-peaked Balmer emission lines originate.
Some correlations between FeII emission lines and the other broad emission
lines for normal AGN can be confirmed for dbp emitters. However, these
results should be taken with caution due to the small number of objects and
the bias in selecting strong FeII emitters. We show that for dbp emitters,
BH masses seems to have more influence on FeII properties than
dimensionless accretion rate.}
{ Accepted by Rev. Mex. A\&A }
{E-mail contact: xguang@astroscu.unam.mx,\newline preprint available at
http://arxiv.org/abs/astro-ph/0610432}
\vspace*{0.6cm}
{\large\bf{The sizes of BLRs and BH masses of double-peaked broad low-ionization
emission line objects}}
{\bf{ Xue-Guang Zhang$^{1,2}$, Dultzin-Hacyan D.$^1$ \ and Ting-Gui Wang$^2$ }}
$^1$ {Instituto de Astronom\'ia, Universidad Nacional Aut\'onoma de
M\'exico, Apdo Postal 70-264, M\'exico D. F. 04510, Mexico} \\
$^2$ {Center for Astrophysics, Department of astronomy and Applied
Physics, University of Science and Technology of China,
Hefei, Anhui, P.R.China}
{ In this paper, the sizes of the BLRs and BH masses of DouBle-Peaked broad
low-ionization emission line emitters (dbp emitters) are compared using
different methods: virial BH masses vs BH masses from stellar velocity
dispersions, the size of BLRs from the continuum luminosity vs the size of
BLRs from the accretion disk model. First, the virial BH masses of dbp
emitters estimated by the continumm luminosity and line width of broad
H$\beta$ are about six times (a much larger value, if including another dbp
emitters, of which the stellar velocity dispersions are traced by the line
widths of narrow emission lines) larger than the BH masses estimated from
the relation $M_{BH} - \sigma$ which is a more accurate relation to
estimate BH masses. Second, the sizes of the BLRs of dbp emitters estimated
by the empirical relation of $R_{BLR} - L_{5100\AA}$ are about three times
(a much larger value, if including another dbp emitters, of which the
stellar velocity dispersions are traced by the line widths of narrow
emission lines) larger than the mean flux-weighted sizes of BLRs of dbp
emitters estimated by the accretion disk model. The higher electron density
of BLRs of dbp emitters would be the main reason which leads to smaller
size of BLRs than the predicted value from the continuum luminosity.}
{ Accepted by MNRAS }
{E-mail contact: xguang@astroscu.unam.mx,\newline preprint available at
http://arxiv.org/abs/astro-ph/0701657}
\vspace*{0.6cm}
{\large\bf{Ly$\alpha$ excess in high redshift radio galaxies: a
signature of star formation.}}
{\bf{M. Villar-Mart\'\i n$^1$, A. Humphrey$^2$, C. De Breuck$^3$,
R. Fosbury$^4$, L. Binette$^2$ and
J. Vernet$^3$}}
$^{1}$ {Instituto de Astrof\'\i sica de Andaluc\'\i a (CSIC), Aptdo.
3004, 18080 Granada, Spain}\\
$^{2}$ {Instituto de Astronom\'\i a, UNAM, Ap. 70-264, 04510, DF,
M\'exico}\\
$^{3}$ {European Southern Observatory, Karl Schwarschild Str. 2, D-85748
Garching bei M\"unchen, Germany}\\
$^{4}$ {ST-ECF, Karl Schwarzschild Str. 2, D-85748 Garching bei
M\"unchen, Germany}
{ About 54\% of radio galaxies at $z\ge$3 and 8\% of radio galaxies at
2$\le z$2.5 radio galaxies. The enhanced star formation
activity in LAEs could be a consequence of a recent merger which has
triggered both the star formation and the AGN/radio activities.
The measurement of unusually high Ly$\alpha$ ratios in the extended gas of
some high redshift radio galaxies suggests that star formation activity
occurs in spatial scales of tens of kpc.
We argue that, although the fraction of LAEs may be incompletely
determined, both at 2$\le z<3$ and at $z\ge3$, the much larger fraction of
LAEs found at $z\ge$3 is a genuine redshift evolution and not due to
selection effects. Therefore, our results suggest that the radio galaxy
phenomenon is more often associated with a massive starburst at $z>$3 than
at $z$100 kpc), which have been for more than
two decades valuable sources of information about the evolutionary status
of the host galaxy and its chemical enrichment and star formation
histories.
I present in this paper a summary of the most relevant results about the
giant nebulae obtained in the last $\sim$10 years and the implications on
our understanding of the early phases of evolution of massive elliptical
galaxies. An interesting earlier review can be found in McCarthy (1993).}
{Presented at the workshop on The Fate of the Gas in Galaxies, Dwingeloo,
The Netherlands, July 2006. To appear in New Astronomy Reviews.}
{E-mail contact: montse@iaa.es,\newline preprint available at
http://babbage.sissa.it/abs/astro-ph/0611763}
%\vspace*{0.6cm}
\newpage
{\large\bf{Chemical enrichment of the intracluster medium by FR~II radio
sources}}
{\bf{ David Heath$^1$, Martin Krause$^1$ \ and Paul Alexander$^1$ }}
$^1$ {Astrophysics Group, Cavendish Laboratory, Cambridge CB3 0HE, UK} \\
{We present 2D axisymmetric hydrodynamic simulations investigating the long
term effect of FR~II radio galaxies on the metal distribution of the
surrounding intra-cluster medium (ICM). A light jet is injected into a
cooling flow atmosphere for $10-30$~Myr. We then follow the subsequen
evolution for $3\,$Gyr on a spherical grid spanning 3~Mpc in radius. A
series of passive tracer particles were placed in an annulus about the
cluster core to simulate metal carrying clouds in order to calculate the
metallicity ($Z$) as a function of time and radial distance from the
cluster centre. The jet has a significant effect on the ICM over the entire
$3\,$Gyr period. By the end of the simulations, the jets produced
metallicities of $\approx ~10$\% of the initial metallicity of the cluster
core throughout much of the cluster. The jets transport the metals not only
in mixing regions, but also through upwelling IC behind the jet, enriching
the cluster over both long and short distances.}
{ Accepted by MNRAS, preprint: astro-ph/0610309}
{E-mail contact: M.Krause@mrao.cam.ac.uk}
\vspace*{0.6cm}
{\large\bf{Line Variability in the High-Resolution X-Ray Spectrum of MCG
-6-30-15}}
{\bf{ Robert R. Gibson$^1$, Claude R. Canizares$^1$, Herman L. Marshall$^1$,
Andrew J. Young$^1$, \ and Julia C. Lee$^2$ }}
$^1$ {MIT Kavli Institute for Astrophysics and Space Research,
Cambridge, MA} \\
$^2$ {Harvard-Smithsonian Center for Astrophysics, Cambridge, MA}
{The recent 540 ks Chandra HETGS spectrum of the well-studied, variable
active galactic nucleus (AGN) \mbox{MCG -6-30-15} shows strong $1s-2p$
absorption lines from many ions. The spectrum was obtained over a period of
about 10 days, and the large number of counts in the spectrum makes it
ideal for testing variability on short timescales. We apply quantitative
tests for line variability to the $1s-2p$ absorption lines of H- and
He-like Ne, Mg, Si, and S. We find significant correlations and
anticorrelations between lines as a function of time, much as we would
expect if ionization levels in the absorber were varying. We also find
evidence for variation in at least one $1s-2p$ resonance absorption line as
a function of luminosity. We consider several possibilities to explain the
line variation. First we consider factors that could change ionization
levels in the absorber: radial motion, density variation, luminosity
variation, and continuum shape variation. None of these individually can
explain the line variation, although we cannot completely constrain
continuum shape variation without simultaneous knowledge of the ultraviolet
(UV) continuum. Other factors, considered individually, are also unable to
explain all the variation: multiple changing continuum components, variable
obscuration, and changes in velocity dispersion. Changes in line emission
are an unlikely cause of significant variation in absorption-line
measurements, but we are unable to fully constrain them. Variability could
be due to a changing line of sight through a structured absorber. Modeling
such scenarios should produce useful constraints on continuum emission
mechanisms and absorber structure.}
{ Published in ApJ, 655:749-761, 2007 February 1 }
{E-mail contact: rgibson@astro.psu.edu}
\vspace*{0.6cm}
{\large\bf{Giant Ly$\alpha$ nebulae around z$>$2 radio galaxies: evidence
for infall}}
{\bf{ A. Humphrey$^1$, M. Villar-Mart\'\i n.$^{2}$, R. Fosbury$^{3}$, L. Binette$^{1}$, J. Vernet$^{4}$, C. De Breuck$^{4}$, \ and S. di Serego Alighieri$^{5}$}}
$^{1}$Instituto de Astronom\'\i a, UNAM, Ap. 70-264, 04510 M\'exico, DF,
M\'exico\\
$^{2}$Instituto de Astrof\'\i sica de Andaluc\'\i a (CSIC), Aptdo. 3004,
18080 Granada, Spain\\
$^{3}$ST-ECF, Karl-Schwarzschild Str. 2, 85748 Garching bei M\"unchen,
Germany\\
$^{4}$European Southern Observatory, Karl Schwarschild Str, 2, D-85748
Garching bei M\"unchen, Germany\\
$^{5}$INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5,
I-50125 Firenze, Italy
{We present an investigation into the possible relationship between
side-to-side asymmetries of powerful radio galaxies at high redshift, with
the goal of understanding the geometry, orientation and gas dynamics of
these sources. Our sample consists of 1 1 radio galaxies at
2.3$\le$z$\le$3.6 previously known to have giant, kinematically quiescent
nebulae. We identify several correlated asymmetries: on the side of the
brightest radio jet and hotspot (i) the redshift of the kinematically
quiescent nebula i s highest, (ii) Ly$\alpha$ is brighter relative to the
other lines and continuum, (iii) the radio spectrum is flattest and (iv)
the radio structure has its highest polarization. These asymmetries are
not found to be correlated with either the radio arm l ength asymmetry or
the brightness asymmetry of the UV-optical emitting material. The
correlation between the radio brightness asymmetry and the radial velocity
of the quiescent gas also appears to be present in powerful radio galaxies
with 0$\le$z$\le$1.
Collectively, these asymmetries are most naturally explained as an effect
of orientation, with the quiescent nebulae in infall: this is the first
study to distinguish between the rotation, infall, outflow and chaotic
motion scenarios for the kinematically quiescent emission line nebulae
around powerful active galactic nuclei.}
{ Accepted by MNRAS }
{E-mail contact: ahumphre@astroscu.unam.mx,\newline preprint available at
http://xxx.lanl.gov/abs/astro-ph/0611778}
\vspace*{0.6cm}
{\large\bf{The Environment of Local Ultraluminous Infrared Galaxies}}
{\bf{B. A. Zauderer$^1$, S. Veilleux$^1$ \ and H.K.C. Yee$^2$ }}
$^1$ {Department of Astronomy, University of Maryland, College Park, MD
20470}\\
$^2$ {Department of Astronomy and Astrophysics, University of Toronto,
Toronto, ON M5S 3H4, Canada}
{The spatial cluster-galaxy correlation amplitude, $B_{gc}$, is computed
for a set of 76 $z < 0.3$ ultraluminous infrared galaxies (ULIRGs) from the
1-Jy sample. The $B_{gc}$ parameter is used to quantify the richness of the
environment within 0.5 Mpc of each ULIRG. We find that the environment of
local ULIRGs is similar to that of the field with the possible exceptions
of a few objects with environmental densities typical of clusters with
Abell richness classes 0 and 1. No obvious trends are seen with redshift,
optical spectral type, infrared luminosity, or infrared color
($f_{25}/f_{60}$). We compare these results with those of local AGNs and
QSOs at various redshifts. The 1-Jy ULIRGs show a broader range of
environments than local Seyferts, which are exclusively found in the field.
The distribution of ULIRG $B_{gc}$-values overlaps considerably with that
of local QSOs, consistent with the scenario where some QSOs go through a
ultraluminous infrared phase. However, a rigorous statistical analysis of
the data indicates that these two samples are not drawn from the same
parent population. The $B_{gc}$ distribution of QSOs shows a distinct tail
at high $B_{gc}$-values which is not apparent among the ULIRGs. This
difference is consistent with the fact that some of the QSOs used for this
comparison have bigger and more luminous hosts than the 1-Jy ULIRGs.}
{ Accepted for publication in the Astrophysical Journal, v660n1 (May
1, 2007).}
{E-mail contact: azaudere@astro.umd.edu or veilleux@astro.umd.edu,\newline
preprint available at http://arxiv.org/abs/astro-ph/0701239}
\vspace*{0.6cm}
{\large\bf{Stratified Quasar Winds: Integrating X-ray and Infrared Views
of Broad Absorption Line Quasars}}
{\bf{S. C. Gallagher$^1$ \& J. E. Everett$^2$}}
$^1$ {Department of Physics \& Astronomy, University of California --
Los Angeles, Los Angeles, CA 90095--1547, USA} \\
$^2$ {Departments of Astronomy \& Physics, and Center for Magnetic
Self-Organization, University of Wisconsin -- Madison, Madison, WI
53706--1390, USA}
{Quasars are notable for the luminous power they emit across decades in
frequency from the far-infrared through hard X-rays; emission at different
frequencies emerges from physical scales ranging from AUs to parsecs. Each
wavelength regime thus offers a different line of sight into the central
engine and a separate probe of outflowing material. Therefore, obtaining a
complete accounting of the physical characteristics and kinetic power of
quasar winds requires a panchromatic approach. X-ray and infrared studies
are particularly powerful for covering the range of interesting physical
scales and ionization states of the outflow. We present a stratified wind
picture based on a synthesis of multiwavelength research programs designed
to constrain the nature of mass ejection from radio-quiet quasars. This
wind comprises three zones: the highly ionized shielding gas, the UV broad
absorption line wind, and the cold dusty outflow. The primary launching
mechanism for the wind likely varies in each zone. While radiative
acceleration on resonance lines dominates for the UV absorbing wind, the
shielding gas may instead be driven by magnetic forces. Ultraviolet
continuum radiative pressure, perhaps coupled with magnetic launching,
accelerates a dusty outflow that obscures the inner broad line region in
unification schemes.}
{To appear in ``The Central Engine of Active Galactic Nuclei,'' ed. L.C. Ho
and J.-M. Wang (San Francisco: ASP).}
{E-mail contact: sgall@astro.ucla.edu,\newline preprint available at
http://arxiv.org/abs/astro-ph/0701076}
%\vspace*{0.6cm}
\newpage
{\large\bf{Response of the warm absorber cloud to a variable nuclear flux
in active galactic nuclei}}
{\bf{Lo\"{i}c Chevallier$^{1,2}$, Bozena Czerny$^2$, A.~R\' o\. za\'
nska$^2$, Anabela C. Gon\c{c}alves$^{1,3}$}}
$^1$ {LUTH, Paris Observatory, 5 place Jules Janssen, F-92195 Meudon
Cedex, France} \\
$^2$ {CAMK, Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716
Warsaw, Poland} \\
$^3$ {CAAUL, Lisbon Observatory, Tapada da Ajuda, 1349-018 Lisboa, Portugal}
{Recent modeling of the warm absorber in active galactic nuclei has proved
the usefulness of constant total (gas plus radiation) pressure models,
which are highly stratified in temperature and density. We explore the
consistency of those models when the typical variation of the flux from the
central source is taken into account. We perform a variability study of the
warm absorber response, based on timescales and our photoionization code
\textsc{TITAN}. We show that the ionization and recombination timescales
are much shorter than the dynamical timescale. Clouds very close to the
central black hole will maintain their equilibrium since the characteristic
variability timescales of the nuclear source are longer than cloud
timescales. For more distant clouds, the density structure has no time to
vary, in response to the variations of the temperature or ionization
structure, and such clouds will show the departure from the constant
pressure equilibrium. We explore the impact of this departure on the
observed properties of the transmitted spectrum and soft X-ray variability:
(i) non uniform velocities, of the order of sound speed, appear due to
pressure gradients, up to typical values of 100 km s$^{-1}$. These
velocities lead to the broadening of lines. This broadening is usually
observed and very difficult to explain otherwise. (ii) Energy-dependent
fractional variability amplitude in soft X-ray range has a broader hump
around $\sim$ 1--2 keV, and (iv) the plot of the equivalent hydrogen column
density vs. ionization parameter is steeper than for equilibrium clouds.
The results have the character of a preliminary study and should be
supplemented in the future with full time-dependent radiation transfer and
dynamical computations.}
{Accepted by A\&A.}
{E-mail contact: loic.chevallier@obspm.fr,\newline preprint available at
http://arxiv.org/abs/astro-ph/0701112}
\vspace*{0.6cm}
{\large\bf{Night-to-night variation in the emission lines of the nucleus
spectrum of the Seyfert galaxy NGC 3227}}
{\bf{ L.P.Metik, I.I.Pronik and L.M.Sharipova }}
{Crimean Astrophysical Observatory, Naudhny, Crimea, Ukraine}
{The results of the emission line study of the optical spectrum of the
Seyfert galaxy NGC 3227 nucleus are presented. 53 spectra obtained during
the maximum nucleus brightness on 12-15 January 1977 with the 6 m telescope
were the basis of the investigations. It was shown that the profilers of
the hydrogen lines broadening during 3 days. The amounts of broadening at
the 0.5 intensity level of H$_\alpha$, H$_\beta$ and H$_gamma$ line profile
peaks were 12\%, 35\% and 44\% respectively. The H$_\beta$ line profile
broadening was accompanied by a decrease in its equivalent width
EW$_\beta$. The increase in the equivalent width EW$_{[OIII]}$ of the
[OIII] line during 3 days was more than 3$\sigma$. It was assumed that a 3
day flare is observed in the galaxy nucleus, which could be caused by shock
in long-lived flows from the galaxy nucleus}
{ Accepted by Astronomical and Astrophysical Transactions }
{E-mail contact: ipronik@crao.crimea.ua,}
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{
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